Relativistic iron emission lines in neutron star low-mass X-ray binaries as probes of neutron star radii

被引：133

作者：

Cackett, Edward M. ^{[1
]}

Miller, Jon M. ^{[1
]}

Bhattacharyya, Sudip ^{[2
,3
]}

Grindlay, Jonathan E. ^{[4
]}

Homan, Jeroen ^{[5
]}

Van Der Klis, Michiel ^{[6
]}

Miller, M. Coleman ^{[3
]}

Strohmayer, Tod E. ^{[7
]}

Wijnands, Rudy ^{[6
]}

机构：

[1] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[2] NASA, Goddard Space Flight Ctr, CRESST & Astrophys Sci Div, Greenbelt, MD 20771 USA

[3] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[4] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[5] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA

[6] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands

[7] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA

来源：

ASTROPHYSICAL JOURNAL | 2008年 / 674卷 / 01期

关键词：

accretion; accretion disks; stars : neutron; X-rays : binaries;

D O I：

10.1086/524936

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Using Suzaku observations of three neutron star low-mass X-ray binaries ( Ser X-1, 4U 1820-30, and GX 349+2) we have found broad, asymmetric, relativistic Fe K emission lines in all three objects. These Fe K lines can be well fit by a model for lines from a relativistic accretion disk ("diskline''), allowing a measurement of the inner radius of the accretion disk and hence an upper limit on the neutron star radius. These upper limits correspond to 14.5-16.5 km for a 1.4 M-circle dot neutron star. The inner disk radii that we measure with Fe K lines are in good agreement with the inner disk radii implied by kHz QPOs observed in both 4U 1820-30 and GX 349+2, supporting the inner disk origin for kHz QPOs. In addition, the Fe K lines observed in these neutron stars are narrower than those in the black holes that are thought to be close to maximally spinning, as one would expect if inferences for spin are robust.

引用

页码：415 / 420

页数：6

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